adsabs/AstroCLIMB huggingface dataset:
Paper: Formation and Eruption of Hot Channels during an M6.5 Class Solar Flare
Authors: Yanjie Liu, Yingna Su, Rui Liu, Jialin Chen, Tie Liu, Haisheng Ji
Figure caption: (a) Magnetic field lines derived from the NLFFF at 17:34:25 UT in 3D perspectives, the cross section of the X–Z plane is the same as those in Figure 6(f). The cyan, pink, and yellow field lines represent the flux ropes passing through the three regions with T  w  ≤ −1.75. The FOV of images in panels (d)–(h) is marked by the white box in Figure 6(a). (b)–(c) Images in AIA 131 Å at 17:22:32 and 17:55:23 UT, and the green boxes represent the FOV of images in panels (d)–(h), and the magenta arrows H1 and H2 represent the two observed hot channels. The yellow and red contours in panel (b) show the photospheric positive and negative magnetic fields taken by SDO/HMI at 17:22:30 UT. (d)–(h) Magnetic field lines superimposed on HMI LOS images at 17:22:25, 17:34:25, 17:46:25, 17:58:25, and 18:10:25 UT, respectively. The orange box in panel (d) represents the FOV of the images in Figure 8. The green and purple lines in panel (h) represent the newly formed flux bundles and a new flux rope, respectively.
Paper: Formation and Eruption of Hot Channels during an M6.5 Class Solar Flare
Authors: Yanjie Liu, Yingna Su, Rui Liu, Jialin Chen, Tie Liu, Haisheng Ji
Figure caption: (a)–(c) Decay index distribution in X–Z planes at three different moments. The cyan, pink, yellow, and purple lines refer to the same field lines as those in Figure 7. The blue, green, white contours in panels (a)–(e) refer to the decay index at 1.1, 1.5, and 2, respectively. (d) NLFFF lines superimposed on HMI LOS images at 17:46:25 UT in 3D perspectives, and the orange cross section in the X–Y plane represents the distribution of the decay index above the top of the flux ropes. (e) Top view of the image in panel (d), the arrow S1 marks the position of images in panels (a)–(b) and the arrow S2 marks the position of the image in panel (c). (f) The evolution of magnetic flux in the areas where T  w  ≤ −1 (black) and T  w  ≤ −1.75 (blue) in the region marked by the green box in Figure 7(d), and the evolution of the magnetic flux ratio (magenta) in the areas with T  w  ≤ −1.75 and T  w  ≤ −1. (g) The evolution of the total current of the flux ropes satisfying T  w  ≤ −1.75 (blue) and T  w  ≤ −1 (black) in the region marked by the green box in Figure 7(d).
Paper: Formation and Eruption of Hot Channels during an M6.5 Class Solar Flare
Authors: Yanjie Liu, Yingna Su, Rui Liu, Jialin Chen, Tie Liu, Haisheng Ji
Figure caption: (a) HMI photospheric vector magnetogram at 17:12 UT. The background map is the vertical component of the magnetic field, the intensity of which is represented by the color bar on the right. The blue (positive) and red (negative) arrows represent the horizontal magnetic fields, the strength of which is represented by the length of the arrows. The white rectangle represents the FOV of images in the second row of Figure 7. (b) Temporal evolution of the max (blue) and mean (orange) T  w  in the regions with T  w  ≤ −1.75. (c)–(i) T  w  distributions in the X–Z cross sections along the green line shown in panel (a). The black dotted box in panel (c) frames the FOV of panels (d)–(i). The ranges of Z are 0″–50″ for panel (c) and 16.″25–47.″5 for panels (d)–(i). The labels A and B mark the upper and right regions with T  w  ≤ −1.75. The cyan, pink, and yellow “*” symbols in panel (g) indicate the flux ropes of the same color code in Figure 7. The magenta contours in panels (c)–(i) represent the T  w  of −1.75.
Paper: Formation and Eruption of Hot Channels during an M6.5 Class Solar Flare
Authors: Yanjie Liu, Yingna Su, Rui Liu, Jialin Chen, Tie Liu, Haisheng Ji
Figure caption: Kinking evolution of hot channels. The first row shows the running-difference images in the AIA 131 Å during the evolution of hot channels. Arrows SH1 (orange) and SH2 (yellow) represent two seed hot channels that merge. The insets at the upper right corner of panels (a)–(c) are enlarged portions of the region framed by the magenta boxes in corresponding panels, to better show the merge of the two seed hot channels. The white arrow KHC1 in panel (d) represents the first kinking hot channel formed by merging. The second row presents the original images observed in AIA 131 Å at the same time as those in the first row. The black boxes in panel (f) mark the brightening of the footpoints of the first kinking hot channel. The third row shows the original images observed in AIA 131 Å during the evolution of the second kinking hot channel, the purple boxes in panels (i)–(l) mark the kinking structure of this hot channel.
Paper: Formation and Eruption of Hot Channels during an M6.5 Class Solar Flare
Authors: Yanjie Liu, Yingna Su, Rui Liu, Jialin Chen, Tie Liu, Haisheng Ji
Figure caption: Evolution of T  w  distribution at the left footpoint of the flux ropes. To better show the evolution, only the twist distribution at the location of T  w  ≤ −1 is shown, and the twist values at other locations are set to zero. The magenta contours represent the T  w  at −1.75. The cyan, pink, and yellow fills correspond to the footpoints of the original three flux ropes, respectively. The arrow in panel (f) marks the footpoint of the newly appeared flux bundles.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Density dependence of theoretical level populations for the two most important metastable states of C-like Fe, compared with measured populations. The geometric electron density of the beam is estimated to be ﹩\mathrm{log}{n}_{e}=11.8﹩ (vertical black dashed line). The measurements are consistent with an effective density of ﹩\mathrm{log}{n}_{e}=10.55﹩, which is lower by a factor of 18 (vertical black dotted line). This reflects the fact that the trapped ion cloud has a larger radius than the electron beam, and thus trapped ions only spend a fraction of their time crossing the electron beam. The ion gyroradius corresponding to this density is 150 μm, nearly 4 times larger than the electron-beam radius.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Results for Be-like Ne VII: fluorescence count rate vs. incoming photon energy. Error bars display the 1σ statistical uncertainties. The red curve shows a fit of four Voigt profiles to the line E1 and three other transitions from metastable states. The blue and green dashed curves show the contributions of the 1S0 ground state and the 3 P 2 metastable state from our population model.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Results for Be-like Fe XXIII: fluorescence count rate vs. incoming photon energy. The shown data are binned to 0.2 eV intervals for clarity. Red curve: fit of six Voigt profiles to ground-state transitions in Li-like (u, v), Be-like (E1, E2), and B-like (B) Fe ions. MS originates from the excitation of a metastable state in Be-like Fe XXIII. Dashed curves: contributions of the different initial states derived from our population model. Dashed orange line: fit of experimental background.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Result for C-like Fe XXI: Fluorescence count rate vs. incoming photon energy. Red curve: fit of eight Voigt profiles to ground-state transitions in B-like (B), C-like (C1, C2), and N-like (N) Fe ions. MS1 to MS4 originate from metastable initial states in C-like Fe XXI. Dashed curves: contributions of the different initial states derived from our population model. Dashed orange line: fit of experimental background.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Fractional populations of metastable states of Be-like Ne evaluated as a function of the electron density at an electron-beam energy close to that of our experiment (E = 360 eV). The population of B-like Ne is set to be 40% of the Be-like one. The calculated electron density inside the beam (black dashed line) and the estimated effective electron density seen by the ions (black dotted line) are shown. In these regimes, the dependence of the population of 2s2p 3 P 2 on density is weak.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Comparison of theory and experiment. (a) Difference between calculated and measured transition energies. Background colors indicate different measurement setups and thus different experimental energy calibrations. The dashed lines indicate offsets of 0 eV, 0.1 eV, and 0.2 eV, respectively. (b) Relative deviation of calculated and measured natural line widths. The dotted lines indicate a ±10% deviation.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Dependence of theoretical level population of the 2p2p 3 P 0 state of Be-like Fe on the relative population of B-like Fe (solid black line). We compare this with the measured population (red dashed line) and charge balance (vertical black dashed line).
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Density dependence of the theoretical level populations for metastable states of Be-like Fe. The estimated electron density (black dashed line) and effective electron density (black dotted line) are shown. In the density regime of our experiment, the population of the 2s2p 3 P 0 state is insensitive to the electron density.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Dependence of the theoretical level population of 2p2p 3 P 2 state of Be-like Ne on the relative population of B-like Ne (solid black line). We compare this with the measured population (horizontal red dashed line) and charge balance (vertical black dashed line).
Paper: Solar Energetic Particle Acceleration at a Spherical Shock with the Shock Normal Angle ﹩{\theta }_{{B}_{n}}﹩ Evolving in Space and Time
Authors: Xiaohang Chen, Joe Giacalone, Fan Guo
Figure caption: Energy spectra at the west (W60° ± 2°) and east (E60° ± 2°) flanks of the shock as well as shock nose (0° ± 2°) when the shock radius reaches (a) 10 R ⊙, (b) 30 R ⊙, (c) 100 R ⊙, and (d) 1 au. The top three panels present the number density of SEPs detected at different locations along the shock front as a function of particle's energy and the time after injection. The button panel shows the corresponding energy spectra of the particles in the top three panels. The dashed lines provide a reference of the flattest and steepest spectra among a certain energy range.
Paper: Solar Energetic Particle Acceleration at a Spherical Shock with the Shock Normal Angle ﹩{\theta }_{{B}_{n}}﹩ Evolving in Space and Time
Authors: Xiaohang Chen, Joe Giacalone, Fan Guo
Figure caption: The spatial distribution of SEPs with energy E > 10 MeV as the shock propagates in the Parker spiral magnetic field (gray lines) at different shock radius R  sh : (a) 3 R ⊙, (b) 10 R ⊙, (c) 30 R ⊙, (d) 100 R ⊙, and (e) 1 au. The red “x” indicates the shock center, fixed at x  sh  = 2 R ⊙ and the black dashed circle presents the position of shock front.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: SANE accretion flows spin up BHs while the MAD state reduces the BH spin magnitude over long timescales. We show the spinup parameter s (Equation (33)) for the MAD and SANE models (cyan circles) in the present work. For comparison, we also show the s for KORAL simulations of MADs (blue circles; Narayan et al. 2022) and SANE disks (orange circles) with nine different BH spins, and H-AMR MAD (magenta circles) and SANE (gray circles) simulations from Event Horizon Telescope Collaboration et al. (2022). The black solid line indicates the spinup parameter for a standard thin disk (Shapiro 2005).
Paper: Solar Energetic Particle Acceleration at a Spherical Shock with the Shock Normal Angle ﹩{\theta }_{{B}_{n}}﹩ Evolving in Space and Time
Authors: Xiaohang Chen, Joe Giacalone, Fan Guo
Figure caption: IMF topology associated with a CME-driven shock in the regions (a) near the Sun and (b) at 1 au.
Paper: Solar Energetic Particle Acceleration at a Spherical Shock with the Shock Normal Angle ﹩{\theta }_{{B}_{n}}﹩ Evolving in Space and Time
Authors: Xiaohang Chen, Joe Giacalone, Fan Guo
Figure caption: The magnetic-field lines in the upstream and downstream of the shock at (a) R  sh  = 3 R ⊙ and (b) R  sh  = 1 au.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We calculate the radial slope of the mass outflow rates ﹩{\dot{M}}_{\mathrm{out}}\propto {r}^{m}﹩ for both the average and instantaneous mass outflow rates (see Figure 7). The slope m is used to determine the radial density profile according to the ADIOS model and is roughly 1 around the inflow equilibrium radius (r ∼ 100r g). However, we caution that ﹩{\dot{M}}_{\mathrm{out}}﹩ drops rapidly as we approach the BH, and therefore, the slope in this region may not have much relevance.
Paper: Solar Energetic Particle Acceleration at a Spherical Shock with the Shock Normal Angle ﹩{\theta }_{{B}_{n}}﹩ Evolving in Space and Time
Authors: Xiaohang Chen, Joe Giacalone, Fan Guo
Figure caption: The schematics of (a) the MHD Rankine–Hugoniot conditions and (b) the geometry used for solving the downstream magnetic field.
Paper: Solar Energetic Particle Acceleration at a Spherical Shock with the Shock Normal Angle ﹩{\theta }_{{B}_{n}}﹩ Evolving in Space and Time
Authors: Xiaohang Chen, Joe Giacalone, Fan Guo
Figure caption: The injection position of high-energy particles (>10 MeV) observed at 1 au. The white “X” denotes the location of shock center.
Paper: Lost in Space: Companions’ Fatal Dance around Massive Dying Stars
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Upper panel: radial density profile of the core and envelope at three phases t 0 < t 1 < t 2 of SN II explosion. Density is normalized with the initial core density. Lower panel: time evolution of the total mass residing inside the secondary’s orbit for expansion velocities 1000, 5000, and 10,000 km s−1.
Paper: Lost in Space: Companions’ Fatal Dance around Massive Dying Stars
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Groups of panels 1–4 show the final orbital parameters a, e, and component velocities as a function of ν assuming a 1 M ⊕ secondary. The applied ejecta speed and initial eccentricity are given. Colors show different a init values. Regions absent of data points (indicated with dashed lines) represent bound models on component velocity panels.
Paper: Lost in Space: Companions’ Fatal Dance around Massive Dying Stars
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Histograms of the eccentricities and the final velocities of the neutron star and companion in the case where the planets (upper panels) and stars (lower panels) become unbound. Different colors represent different secondary masses, also indicated in the key. Different populations can be distinguished, whose width increases with M sec. The gray areas show completely overlapping regions.
Paper: Lost in Space: Companions’ Fatal Dance around Massive Dying Stars
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Distribution of the primary and secondary velocities of unbound planets (panels a and b) and stellar-mass companions (panels c and d) by the end of the simulation. Colors represent secondary mass on the left and initial true anomaly on the right panels. Values of v pri are on a wide range and thus shown on a logarithmic scale, while v sec values are on a linear scale.
Paper: Lost in Space: Companions’ Fatal Dance around Massive Dying Stars
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Histograms of the orbital parameters (top two rows: a, bottom two rows: e for planets and stars, respectively) of bound systems at the end of integration. Panels show cases with different M n values. Colors represent different M ej values, also shown in the key.
Paper: Lost in Space: Companions’ Fatal Dance around Massive Dying Stars
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Representative eccentricity evolution models for planetary (a) and stellar (b) systems. Solid lines represent unbound systems, while dotted (e < e init) and dotted–dashed (e > e init) lines represent bound systems. Colors represent different e init values, which are exactly the same for a given color. For visibility, we use a logarithmic scale in panel (a).
Paper: Lost in Space: Companions’ Fatal Dance around Massive Dying Stars
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Same as Figure 5 for a stellar companion of 5 M ⊙.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Redshift distributions of the BBHs observed at ET alone in 1 yr, selected on the basis of different thresholds for the S/N (left panel), or setting S/N ≥ 12 and applying further cuts on Δd  L /d  L  (central panel), or on ΔΩ90% (right panel). The black solid line corresponds to the total BBH population in the astrophysical model that we have assumed. We set ﹩{{ \mathcal R }}_{0,\mathrm{BBH}}=17\,{\mathrm{Gpc}}^{-3}\,{\mathrm{yr}}^{-1}﹩, and show the results for the detections in 1 yr (taking into account our assumptions of the duty cycle). In each column, the upper panel shows the number of events per redshift bin, while the lower panel shows the corresponding cumulative distributions, normalized to the number of BBH events in our sample, N BBH = 7.5 × 104.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Detection horizons for different monochromatic populations of BBH sources for the LVK detector network during O4, for ET alone, and for a network of two CE detectors (without ET), taken one with 40 km arms and one with 20 km arms. The solid lines show the maximum redshift out to which a binary with optimal sky location and inclination can be detected, while the shaded bands represent the maximum z out to which a binary could be observed after averaging the S/N over the sky, which is a proxy for the redshift out to which 50% of the population with given masses and spins could be detected. We set a detection threshold S/N = 8. In the left panel, we show the result for equal-mass nonspinning binaries; in the central panel, for nonspinning binaries with a mass ratio q = 5; and in the right panel, for binaries with a mass ratio q = 5 and aligned spin components χ 1,z  = χ 2,z  = 0.8. We use the IMRPhenomHM waveform.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Scatter plots of the observed BBH population at the various networks. In the first row, we show the results for the LVK network in O4; in the middle, for ET alone; and in the bottom, for the ET+2CE network. In each row, the left panel shows the distribution of errors on the luminosity distance and sky location, with the color code representing the redshift, the central panel, the distribution of errors on the luminosity distance, and detector-frame chirp mass, again with the color code representing the redshift; and the right panel, the distribution of errors on the source-frame chirp mass and symmetric spin χ  s  = (χ 1 + χ 2)/2, with the color code representing the total source-frame mass. The numbers reported on the dashed lines refer to the fraction of observed events lying inside the corresponding region.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Cumulative distributions of the number of detections per year, for the S/Ns and for the error on the parameters, for BBH signals with the three considered network configuration, using the waveform model IMRPhenomHM, and the value ﹩{{ \mathcal R }}_{0,\mathrm{BBH}}=17\,{\mathrm{Gpc}}^{-3}\,{\mathrm{yr}}^{-1}﹩ for the local rate. Except for the panel showing the distribution of the S/N, only the events whose Fisher matrix could be reliably inverted are included.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: As in Figure 10, for ET+2CE.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: As in Figure 4 for NSBH sources. The NS mass is fixed to m NS = 1.33 M ⊙ while we vary the BH mass in the astrophysically motivated range [3, 30] M ⊙ (Broekgaarden et al. 2021). In the left panel, we show the results for nonspinning binaries neglecting tidal effects; in the central panel, for binaries having a BH with aligned spin component χ BH,z  = 0.8; and in the right panel, we consider both the effect of a spinning BH with χ BH,z  = 0.8 and a tidal deformability parameter for the NS Λ = 360, which is consistent with the APR4 (Akmal et al. 1998) soft equation of state. We use the waveform model IMRPhenomNSBH.